My research focus is on the nuclear physics required to understand the mechanisms responsible for production of heavy nuclei in explosive stellar environments. The main part of the experimental efforts is to directly measure the cross sections for nuclear reactions that are key for the stellar p-process. However, since only a fraction of all the required reactions is experimentally accessible, tools that can predict the required cross sections are necessary. One such tool, statistical models, require information about the nuclear properties, such as level densities and gamma-strength functions to calculate the reaction cross sections. These nuclear properties are modeled with large uncertainties that propagate to the resulting cross sections. To reduce these uncertainties, I utilize the Oslo method to extract the statistical nuclear properties from experimental data. Finally, I use the cross sections obtained from the above methods to investigate the impact of the new reaction cross sections on the abundances of the nuclei produced by the p-process.

Follow the links below to learn more about the research efforts of my group:

Hauser-Feshbach calculations

Understanding the p-process requires not only information on the stellar environment in which the process takes place, but also input from nuclear physics. The latter includes nuclear masses, half-lives of the unstable nuclei and rates of all the reactions involved. The p-process is a network of (γ,p), (γ,α) and (γ,n) reactions and their inverse on …

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HECTOR (High Efficiency TOtal absorption spectrometeR) is a NaI(Tl) detector that has been developed at NSL and build by St. Gobain Crystals. It is an array of 16 crystals, each 4x8x8 inches in size. Each crystal is contained in an aluminum housing and read by two photomultipliers. The crystals are arranged in a frame to …

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Level densities and gamma-strength functions

Stellar nucleosynthesis processes involve thousands of reactions for which the cross sections need to be described using theoretical models. For a wide variety of processes, e.g. p-, s- and r- process the nucleosynthesis path runs through heavy nuclei, thus statistical Hauser-Feshbach (HF) models can be applied to describe the cross sections. HF models requires as …

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Network calculations

libnucnet is a collection of libraries developed at Clemson University by Brad Meyer and his collaborators for network calculation application. It is available under the GNU General Public License. Information about the code can be found here: NucNet-Tools is a set of codes based on libnucnet for post-processing network calculations. It provides tools useful …

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The p-process occurs in oxygen-neon burning layers of the Supernova, where, during earlier evolution stages, the neutron-rich nuclei were produced by the s-process. During the SN explosion, gamma-rays traverse through the SN layers destroying the s-nuclei during a series of (γ,n) reactions. The abundances shift towards proton rich nuclei, which undergo further photodisintegration via (γ,p) …

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